Besides the detection of emission coincident with the DLA position,
our PCWI search has allowed us to trace the environment of this DLA
out to 80 kpc. However, apart from the detection of a fairly bright DLA host, no other galaxies are seen in the field, to a luminosity limit of \(5.3 \times 10^{41} \rm erg\ s^{-1}\) .
This is a somewhat rare occurrence compared to previous studies that have examined the large-scale environment of DLAs. For instance, efforts to directly image the DLA host galaxies show a very small probability of DLAs being associated with bright Lyman-break galaxies at distances \(<10-20~\rm kpc\) .
These studies favour instead associations with either faint, possibly isolated, star-forming galaxies or dwarf galaxies which are clustered with more massive LBGs
[1]}.
Moreover, in a recent MUSE
survey of 6 high redshift (\(z > 3\) ) quasar sightlines with
H i column density ranging between 20.3 \(\le \)  log\(N\)(H i)\( \rm [cm^{-2}] \le 21.15\) 
[2]} have traced the environment of
DLA host galaxies out to 250 kpc, detecting 5 high-confidence Ly\(\alpha \)  emitting galaxies associated with three DLAs and 9 lower-significance Ly\(\alpha \)  emission objects in five sightlines.
The MUSE detections are typically found at relatively large impact parameters of \(> 50\)  kpc, implying that DLAs generally trace the neutral gas in a wide variety of rich environments, including overdense structures with multiple members.
